Exploring cosmic origins with CORE: mitigation of systematic effects

Natoli, P.; Ashdown, M.; Banerji, R.; Borrill, J.; Buzzelli, A.; de Gasperis, G.; Delabrouille, J.; Hivon, E.; Molinari, D.; Patanchon, G.; Polastri, L.; Tomasi, M.; Bouchet, F. R.; Henrot-Versillé, S.; Hoang, D. T.; Keskitalo, R.; Kiiveri, K.; Kisner, T.; Lindholm, V.; McCarthy, D.; Piacentini, F.; Perdereau, O.; Polenta, G.; Tristram, M.; Achucarro, A.; Ade, P.; Allison, R.; Baccigalupi, C.; Ballardini, M.; Banday, A. J.; Bartlett, J.; Bartolo, N.; Basak, S.; Baselmans, J.; Baumann, D.; Bersanelli, M.; Bonaldi, A.; Bonato, M.; Boulanger, F.; Brinckmann, T.; Bucher, M.; Burigana, C.; Cai, Z. -Y.; Calvo, M.; Carvalho, C. -S.; Castellano, G.; Challinor, A.; Chluba, J.; Clesse, S.; Colantoni, I.; Coppolecchia, A.; Crook, M.; D'Alessandro, G.; de Bernardis, P.; De Zotti, G.; Di Valentino, E.; Diego, J. -M.; Errard, J.; Feeney, S.; Fernandez-Cobos, R.; Finelli, F.; Forastieri, F.; Galli, S.; Genova-Santos, R.; Gerbino, M.; Gonzalez-Nuevo, J.; Grandis, S.; Greenslade, J.; Gruppuso, A.; Hagstotz, S.; Hanany, S.; Handley, W.; Hernandez-Monteagudo, C.; Hervias-Caimapo, C.; Hills, M.; Keihänen, E.; Kitching, T.; Kunz, M.; Kurki-Suonio, H.; Lamagna, L.; Lasenby, A.; Lattanzi, M.; Lesgourgues, J.; Lewis, A.; Liguori, M.; López-Caniego, M.; Luzzi, G.; Maffei, B.; Mandolesi, N.; Martinez-Gonzalez, E.; Martins, C. J. A. P.; Masi, S.; Melchiorri, A.; Melin, J. -B.; Migliaccio, M.; Monfardini, A.; Negrello, M.; Notari, A.; Pagano, L.; Paiella, A.; Paoletti, D.; Piat, M.; Pisano, G.; Pollo, A.; Poulin, V.; Quartin, M.; Remazeilles, M.; Roman, M.; Rossi, G.; Rubino-Martin, J. -A.; Salvati, L.; Signorelli, G.; Tartari, A.; Tramonte, D.; Trappe, N.; Trombetti, T.; Tucker, C.; Valiviita, J.; Van de Weijgaert, R.; van Tent, B.; Vennin, V.; Vielva, P.; Vittorio, N.; Wallis, C.; Young, K.; Zannoni, M.

doi:10.48550/arxiv.1707.04224

Cited by 4 publications

(9 citation statements)

References 16 publications

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“…We compare the CORE design with that of other proposals, and discuss the pros and cons of the various options. A number of relevant questions are addressed in companion papers, which investigate in more detail: the scientific case for the mission [13,15,18,24,27,48]; its ability to address contamination of the observations by astrophysical foreground emission [81]; data analysis techniques that can help mitigate systematic effects [51]; and the design of the instrument [22].…”

Section: Jcap04(2018)014mentioning

confidence: 99%

“…Systematics are characterised and corrected for a posteriori, with a global interpretation of the scientific data themselves, marginalising over nuisance parameters that model instrument properties and sources of systematic errors. The elementary tools of the data analysis pipeline are outlined in section 7 and discussed in more detail in one of the companion papers [51]. The spacecraft spins at a rate of order f spin 0.5 RPM, so that the line of sight scans the sky on quasi-circles of opening angle β with a period of about 2 minutes.…”

Section: Jcap04(2018)014mentioning

confidence: 99%

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Exploring cosmic origins with CORE: Survey requirements and mission design

Delabrouille

Bernardis

Bouchet

et al. 2018

J. Cosmol. Astropart. Phys.

155

161

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Future observations of cosmic microwave background (CMB) polarisation have the potential to answer some of the most fundamental questions of modern physics and cosmology, including: What physical process gave birth to the Universe we see today? What are the dark matter and dark energy that seem to constitute 95% of the energy density of the Universe? Do we need extensions to the standard model of particle physics and fundamental interactions? Is the ΛCDM cosmological scenario correct, or are we missing an essential piece of the puzzle? In this paper, we list the requirements for a future CMB polarisation survey addressing these scientific objectives, and discuss the design drivers of the CORE space mission proposed to ESA in answer to the "M5" call for a medium-sized mission. The rationale and options, and the methodologies used to assess the mission's performance, are of interest to other future CMB mission design studies. CORE has 19 frequency channels, distributed over a broad frequency range, spanning the 60-600 GHz interval, to control astrophysical foreground emission. The angular resolution ranges from 2 to 18 , and the aggregate CMB sensitivity is about 2 µK.arcmin. The observations are made with a single integrated focal-plane instrument, consisting of an array of 2100 cryogenically-cooled, linearly-polarised detectors at the focus of a 1.2-m aperture cross-Dragone telescope. The mission is designed to minimise all sources of systematic effects, which must be controlled so that no more than 10 −4 of the intensity leaks into polarisation maps, and no more than about 1% of E-type polarisation leaks into B-type modes. CORE observes the sky from a large Lissajous orbit around the Sun-Earth L2 point on an orbit that offers stable observing conditions and avoids contamination from sidelobe pick-up of stray radiation originating from the Sun, Earth, and Moon. The entire sky is observed repeatedly during four years of continuous scanning, with a combination of three rotations of the spacecraft over different timescales. With about 50% of the sky covered every few days, this scan strategy provides the mitigation of systematic effects and the internal redundancy that are needed to convincingly extract the primordial B-mode signal on large angular scales, and check with adequate sensitivity the consistency of the observations in several independent data subsets. CORE is designed as a "near-ultimate" CMB polarisation mission which, for optimal complementarity with ground-based observations, will perform the observations that are known to be essential to CMB polarisation science and cannot be obtained by any other means than a dedicated space mission. It will provide well-characterised, highly-redundant multi-frequency observations of polarisation at all the scales where foreground emission and cosmic variance dominate the final uncertainty for obtaining precision CMB science, as well as 2 angular resolution maps of high-frequency foreground emission in the 300-600 GHz frequency range, essential for complementarity w...

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Section: Jcap04(2018)014mentioning

confidence: 99%

Section: Jcap04(2018)014mentioning

confidence: 99%

Exploring cosmic origins with CORE: Survey requirements and mission design

Delabrouille

Bernardis

Bouchet

et al. 2018

J. Cosmol. Astropart. Phys.

155

161

View full text Add to dashboard Cite

show abstract

“…The latter is a realization of a fiducial cosmological model 8 with ∆ = 0.37 × 10 −3 Mpc −1 . This treatment assumes ideal component separation and negligible systematic effects at the level experimental efforts [44,47,48,49].…”

Section: Forecasts For Future Experimentsmentioning

confidence: 99%

The evens and odds of CMB anomalies

Gruppuso

Kitazawa

Lattanzi

et al. 2018

Physics of the Dark Universe

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The lack of power of large-angle CMB anisotropies is known to increase its statistical significance at higher Galactic latitudes, where a string-inspired preinflationary scale ∆ can also be detected. Considering the Planck 2015 data, and relying largely on a Bayesian approach, we show that the effect is mostly driven by the even-harmonic multipoles with 20, which appear sizably suppressed in a way that is robust with respect to Galactic masking, along with the corresponding detections of ∆. On the other hand, the first odd -multipoles are only suppressed at high Galactic latitudes. We investigate this behavior in different sky masks, constraining ∆ through even and odd multipoles, and we elaborate on possible implications. We include low-polarization data which, despite being noise-limited, help in attaining confidence levels of about 3 σ in the detection of ∆. We also show by direct forecasts that a future all-sky Emode cosmic-variance-limited polarization survey may push the constraining power for ∆ beyond 5 σ.

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“…Optical scan strategy for CMB polarimetry has been the subject of multiple publications (Delabrouille et al 2000;Dupac & Tauber 2005;Wallis et al 2017;Natoli et al 2017).…”

Section: Scan Strategy Sampling Frequency and Durationmentioning

confidence: 99%

Full-sky beam convolution for cosmic microwave background applications

Duivenvoorden

Gudmundsson

Rahlin

2019

Monthly Notices of the Royal Astronomical Society

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We introduce a publicly available full-sky beam convolution code library intended to inform the design of future cosmic microwave background (CMB) instruments and help current experiments probe potential systematic effects. The code can be used to assess the impact of optical systematics on all stages of data reduction for a realistic experiment, including analyses beyond power spectrum estimation, by generating signal timelines that may serve as input to full analysis pipelines. The design and mathematical framework of the Python code is discussed along with a few simple benchmarking results. We present a simple two-lens refracting telescope design and use it together with the code to simulate a year-long dataset for 400 detectors scanning the sky on a satellite instrument. The simulation results identify a number of sub-leading optical non-idealities and demonstrate significant B-mode residuals caused by extended sidelobes that are sensitive to polarized radiation from the Galaxy. For the proposed design and satellite scanning strategy, we show that a full physical optics beam model generates B-mode systematics that differ significantly from the simpler elliptical Gaussian model. The code is available at https://github.com/adrijd/beamconv.

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Exploring cosmic origins with CORE: mitigation of systematic effects

Cited by 4 publications

References 16 publications

Exploring cosmic origins with CORE: Survey requirements and mission design

Exploring cosmic origins with CORE: Survey requirements and mission design

The evens and odds of CMB anomalies

Full-sky beam convolution for cosmic microwave background applications

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